Sieging HELM's deep: PRIMA unveils the far-infrared properties of highly extincted low-mass galaxies

Carlotta Gruppioni; Giovanni Gandolfi; Giulia Rodighiero; James M.S. Donnellan; Laura Bisigello; L. Y. Aaron Yung; Seb Oliver; Stephen M. Wilkins

REVIEW 3 major objections 3 minor 41 references

Sieging HELM's deep: PRIMA unveils the far-infrared properties of highly extincted low-mass galaxies

T0 review · 3 major / 3 minor · reviewed 2026-08-05 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read This paper predicts that PRIMAger, the far-infrared camera on the proposed PRIMA mission, would detect about 31,000 HELM galaxies in a 1000-hour survey of one square degree, including about 100 at z≈1–1.5, and that about a third would have

desk verdict The paper's core forecast is off by a factor of ten in its own area scaling, and the sensitivity assumptions are optimistic enough that the headline numbers don't stand as written; the qualitative conclusion likely survives. read the letter →

arxiv 2509.01305 v1 pith:HIAWWEOU submitted 2025-09-01 astro-ph.GA astro-ph.IM

Laura Bisigello , Carlotta Gruppioni , Giulia Rodighiero , Giovanni Gandolfi , James M.S. Donnellan , Seb Oliver , Stephen M. Wilkins , L. Y. Aaron Yung This is my paper

classification astro-ph.GAastro-ph.IM

keywords HELMgalaxiesfar-infraredsurveysPRIMAgerdustattenuationmassgalaxyevolutionsurveypredictions

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper asks what a proposed far-infrared space camera, PRIMAger, would see if it stared at one square degree of sky for 1000 hours, targeting a newly identified population of highly extincted low-mass (HELM) galaxies: small galaxies whose dust hides their starlight far more than their stellar masses would suggest. The central claim is that PRIMAger would detect roughly 31,000 HELM galaxies, about 100 of them at redshifts 1–1.5, and that for about a third of the sample the detection in four far-infrared bands between 96 and 235 µm would allow a genuine measurement of dust mass and temperature. If correct, this turns a handful of JWST photometric oddities into a statistically meaningful sample, letting astronomers test whether these galaxies' extreme extinction comes from an unusually large dust reservoir or simply from how they are oriented. The paper's case is that a large-area far-infrared survey, not deeper JWST imaging alone, is the next step for understanding dust production in low-mass galaxies.

What carries the argument

The central machine is the SED-to-PRIMAger flux conversion: each HELM candidate's best-fit optical-to-near-infrared spectral energy distribution is extrapolated into PRIMAger's six far-infrared bands, and a source counts as detected if its predicted flux exceeds three times the survey depth in at least one band. The two named objects doing the work are the HELM selection box (low stellar mass plus high dust attenuation) and PRIMAger's filter set: the 24–84 µm hyperspectral imager and the 96–235 µm broad-band filters.

What would settle it

Re-run the same HELM SED templates and the S/N>3 selection using the confusion-limited 5σ depths quoted in the paper (281 µJy at 96 µm, 747 µJy at 126 µm, 2650 µJy at 172 µm, 7030 µJy at 235 µm) instead of the nominal instrumental depths; if the predicted detection count or the four-filter fraction falls far below 3.1×10^4 and 32%, the central prediction is falsified. A real 1000-hour PRIMAger field over 1 deg² would settle it observationally by counting HELM candidates detected in at least four bands.

Watch

Extended reading notes

Core claim

The paper starts from the HELM candidates selected in a JWST survey field by a companion catalogue, and for each one takes the best-fit spectral energy distribution from a Bayesian SED-fitting code (multiple star-formation histories, two dust attenuation laws, and a dust emission model) to predict fluxes in PRIMAger's bands. For a 1000-hour survey over one square degree and a signal-to-noise threshold of 3, it predicts that PRIMAger would detect about 3.1×10^4 HELM sources in at least one filter, about 100 of them at z=1–1.5, and that 32% of the detected sample would be seen in at least four broad-band filters covering 96–235 µm. The central claim is that this combination—many detections plu

Load-bearing premise

The projected counts assume the camera reaches its nominal sensitivity in the 96–235 µm bands, even though the paper notes that unresolved background sources there create a noise floor brighter than those sensitivities and that deblending has only been demonstrated at flux levels several times brighter.

Editorial extensions

If this is right

A 1000-hour, 1 deg² PRIMAger survey would detect roughly 3.1×10^4 HELM galaxies, two or three orders of magnitude more than the handful currently known, because the wide area compensates for the small fraction of the HELM population that is bright enough.
About 100 of those detections would lie at z=1–1.5, extending the study of dusty low-mass galaxies beyond the mostly z<1 photometric sample.
For the 32% detected in at least four PRIMAger filters (96–235 µm), dust emission fits would yield dust masses and obscured star-formation rates rather than a single detection.
Combined with optical and near-infrared photometry, the multi-band far-infrared data would allow a direct test of whether HELM galaxies' high extinction is caused by a large dust reservoir or by orientation.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

If the demonstrated deblending depths (281–7030 µJy at 96–235 µm) rather than the nominal instrumental depths are adopted, the predicted 3.1×10^4 count and the 32% four-filter fraction would shrink; the paper's headline numbers should be read as an optimistic bound until faint-end source extraction is demonstrated.
The same SED-extrapolation pipeline could be applied to other survey designs or fields with public optical imaging to map how the HELM detection yield trades against area and depth; the paper only explores the 1000-hour, 1 deg² case.
If even a tenth of the predicted detections materialize, stacking analyses could push to the fainter HELM majority and give a first census of dust in low-mass galaxies at z<1.
A realistic end-to-end simulation including confusion noise and deblending at the faint end could calibrate photometric uncertainties for the four-filter subset before launch; the current predictions assume perfect source extraction at the instrument limits.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Colleague,

This is a feasibility forecast for PRIMAger's ability to detect a recently discovered population of low-mass, highly extincted galaxies. The target population is genuinely interesting, and I believe this is the first paper to actually run the numbers for PRIMAger on HELM candidates from JWST. That alone makes it worth reading. The approach is straightforward: take the best-fit BAGPIPES SEDs from Bisigello et al. (in prep.), translate them into predicted PRIMAger fluxes, and compare with a 1000-hour, 1 deg^2 survey. The paper is clearly written, the assumptions are mostly stated, and the qualitative point that PRIMAger should pick up at least some HELM galaxies is almost certainly right.

But the headline number is wrong. Section 3 reports 77 HELM detections in the 90 arcmin^2 CEERS field. That's 0.025 deg^2, so the area scaling to 1 deg^2 is a factor of 40, not 400. The correct extrapolation is ~3.1e3, not 3.1e4. The same error propagates to the abstract, Section 4, and the claim of 100 sources at z=1-1.5 (which should be ~10). This is not a subtle modeling choice; it's an arithmetic slip, and it needs to be fixed before the paper can be taken at face value.

The second issue is the sensitivity assumption. The paper acknowledges that the confusion limit exceeds the instrumental 5σ depths at λ>42.6 µm, and it cites deblending work that recovers sources down to 281–7030 µJy at 96–235 µm. Those are factors of 2.5 to 30 brighter than the instrumental depths used in Table 1. Yet the calculation adopts the instrumental depths, arguing deblending might improve on the classical confusion limit. That is optimistic, and it is especially damaging for the four-filter (PPI1–PPI4) fraction, since the deeper PPI3/PPI4 filters are where the discrepancy is worst. The paper should either use the deblended depths as a baseline, or present a range. As written, the predicted counts and the 32% multi-filter fraction are upper limits, not central expectations.

The qualitative conclusions – that PRIMAger would detect the more massive, less obscured tail of the HELM population, and that a large-area survey is needed – survive both corrections. The paper is also honest about the dependence on ancillary optical data. So this is not a flawed idea; it's a forecast that needs a corrected arithmetic factor and a more conservative sensitivity choice.

I'd send this back for revision rather than reject outright. The errors are fixable, and once corrected, the paper would be a useful reference for the PRIMAger community. It's not a paper with a novel method, but it's a genuinely useful feasibility study for an understudied population.

Hope this helps.

Referee Report

3 major / 3 minor

Summary. This paper uses JWST-based HELM galaxy candidates in the CEERS field, forward-models their SEDs with BAGPIPES to predict PRIMAger fluxes, and compares the predicted fluxes with the 5σ depths of a hypothetical 1000-h/deg² PRIMAger survey. The authors report that 77 HELM sources (2 HELM-3σ, 8 HELM-2σ, 67 HELM-1σ) would be detected in at least one PRIMAger filter and claim this scales to 3.1×10⁴ sources over 1 deg², including ~100 at z=1–1.5, with 32% detected in four filters (PPI1–PPI4). They argue this sample would enable dust-mass and SED characterisation of the HELM population.

Significance. The paper addresses a timely question—whether the proposed PRIMA mission can deliver a statistical sample of the rare, highly obscured low-mass galaxies discovered with JWST. Its strengths are the use of real photometric data in CEERS, a publicly available SED fitting code, and explicit discussion of confusion and deblending limits. The paper makes explicit, testable predictions for PRIMAger detection counts, which is a useful feature for mission planning. However, the headline number is an order of magnitude too high because of an area-scaling error, and the adopted sensitivity is more optimistic than the paper's own confusion/deblending estimates support. With corrected scaling and confusion-limited depths, the predicted sample size and the four-filter fraction are likely to be substantially lower. The scientific conclusion may survive in weakened form, but the quantitative claims need to be redone.

major comments (3)

[Abstract; Section 3 ('Overall, we expect...'), Fig. 4] The headline number is internally inconsistent. The CEERS field is 90 arcmin² = 0.025 deg², so the area factor to 1 deg² is 40. The paper reports 77 HELM detections (2 HELM-3σ + 8 HELM-2σ + 67 HELM-1σ) in that field; 77 × 40 = 3.1×10³, not 3.1×10⁴. The sentence 'The increase in number ... is due to the increase in area, from 90 arcmin² to 1 deg²' cannot yield a factor of 400. The abstract and Section 4 repeat the erroneous 3.1×10⁴. Consequently the 'around 100 sources at z=1–1.5' and the absolute numbers behind the 32% multi-filter statistic must be re-derived.
[Section 3, Table 1 and confusion discussion] The detection calculation adopts the instrumental 5σ depths in Table 1 even though the text states that the 5σ confusion limits exceed these depths at λ>42.6 µm. The deblending simulations cited (Donnellan et al. 2024) give 5σ depths of 281, 747, 2650, and 7030 µJy in PPI1–PPI4, i.e. factors ~2.5–30 brighter than the Table 1 values of 110, 197, 144, 229 µJy. Since the S/N>3 criterion is applied to these depths, the predicted detection numbers and especially the 32% fraction detected in all four PPI filters are optimistic. The speculative statement that other techniques may reduce confusion further does not justify using unverified depths for the baseline forecast. The calculation should be repeated with the demonstrated deblending depths, or at least with a bracketing sensitivity.
[Section 3; Section 2 (SED fitting setup)] The predicted FIR fluxes are taken from the single best-fit BAGPIPES model for each HELM galaxy, with a delayed SFH, Calzetti law, Draine & Li dust, log U in [-4,-2], and q_PAH=2. The FIR flux is therefore an extrapolation from rest-frame optical/NIR photometry with no propagation of the posterior uncertainty. The paper gives no indication of the range in predicted fluxes across the alternative SFHs, extinction laws, or PAH fractions listed in Section 2. Since the detection counts are sensitive to whether a source is above or below the depth threshold, the forecast should include this modelling uncertainty (e.g., using the full posterior or the alternative setups) rather than a single model.

minor comments (3)

[Section 2, Eq. (1)] The logical expression in Eq. (1) is ambiguous: the second conjunction should be parenthesised to show precedence. Also, 'The sample was then cleaned by any source...' should read 'cleaned of any source...'.
[References 40-41] The Euclid overview paper is cited twice (Refs. 40 and 41) with slightly different publication states; these should be combined into a single reference with one consistent citation.
[Section 3, Fig. 2] The dotted lines are described as median SEDs of undetected sources, but the caption and text do not fully specify the redshift binning or the definition of the shaded regions. A clearer caption or legend would improve readability and reproducibility of the figure.

Circularity Check

1 steps flagged · score 4.0 of 10

No tautological reduction; the central prediction is a forward model, but its load-bearing input is the authors' own unpublished HELM catalogue.

self citation load bearing [Section 2 ('Input HELM catalogues'), opening sentence; also Introduction refs 15-18]
"The input HELM sample is taken from Bisigello et al. (in prep.) ... The final catalogues include 2621 HELM-1σ, 174 HELM-2σ, and 17 HELM-3σ objects."

The paper's headline prediction ("about 3.1 × 10^4 HELM sources") is a count of objects defined wholly by the authors' own prior unpublished analysis: the HELM selection, the SED-fitting outputs (M*, AV), and the dust-emission models from which PRIMAger fluxes are extracted all come from the same group. PRIMAger is not used to identify HELM independently; rather, objects are labeled HELM by the self-cited catalogue, and those same model SEDs are then used to predict FIR detectability. Thus the predicted detections inherit the HELM classification rather than test it against FIR data. This is load-bearing: if the prior catalogue or its SED assumptions were wrong, every predicted number would change, and no external validation of the catalogue is offered in the paper. It is not a pure tautolo

full rationale

The paper's derivation chain is: take a HELM catalogue from Bisigello et al. (in prep.), extract PRIMAger fluxes from the same SED fits, compare to assumed depths, and scale counts from CEERS to 1 deg^2. The only circular element is that the catalogue and SEDs originate from the same authors' unpublished work, making the prediction dependent on a self-citation chain for its input. The FIR flux prediction itself is not fitted to PRIMAger data and does not reduce to a fitted parameter, so this is not a tautology. Other concerns in the paper are correctness issues rather than circularity: the 77 detections in 90 arcmin^2 scale to ~3.1e3 per deg^2, not the claimed 3.1e4, and the adopted instrumental 5σ depths are fainter than the paper's own quoted confusion/deblending limits at several wavelengths. These are internal inconsistencies or optimistic assumptions, not reductions of the conclusion into the premises. The paper also transparently notes that only one HELM is spectroscopically confirmed and that the FIR nature is unconstrained, so it does not hide the uncertainty. Overall, some self-citation is load-bearing for the input sample, but the central prediction retains independent forward-modeling content.

Assumptions & free parameters 4 free parameters · 4 assumptions · 0 invented entities

The predicted counts rest on a chain of modeling choices: the hand-drawn HELM selection boundary, the fixed PAH fraction and dust model used to extrapolate FIR fluxes, the assumption that CEERS represents the whole sky, and the optimistic use of instrument noise limits over confusion noise. These are the inputs that drive the headline 3.1e4 number.

free parameters (4)

HELM selection boundary slope and intercept = slope=1.6, intercept=-12.6 (Eq. 1)
Defines which galaxies count as HELM in the companion paper; chosen by hand to separate 'above expectations' extinction from the normal relation. Directly sets the input sample used for all predictions.
PAH mass fraction (q_PAH) = 2
Fixed value in the Draine & Li (2007) dust models used for SED fitting. Affects the predicted FIR SED shape and hence the PRIMAger fluxes; the paper cites prior work for minor impact on stellar mass and AV, but does not quantify the impact on FIR fluxes.
Ionisation parameter range = log10(U) from -4 to -2
Range allowed in the SED fitting, with a best-fit value chosen per source. A modeling choice that affects the nebular continuum and line emission in the fitted SEDs, and thus the extrapolated FIR fluxes.
Dust emission model and SFH choice = Draine & Li (2007), delayed SFH, Calzetti law
The 'best SED model' is selected from several alternatives (delayed, declining, double-power-law SFHs; Calzetti and SMC extinction). The choice of this specific combination for FIR flux extraction is a free modeling decision.

assumptions (4)

standard math The BAGPIPES SED fitting code correctly computes photometric fluxes and physical parameters from the input photometry.
The pipeline uses BAGPIPES (Carnall et al. 2018) as the SED fitting engine; the correctness of its output is assumed without independent verification in this paper.
domain assumption The FIR emission of each HELM candidate is well predicted by the best-fit optical-to-NIR SED model extrapolated with the Draine & Li (2007) dust emission model.
Invoked in Section 3 where fluxes in PRIMAger filters are extracted from the best SED models. If the true FIR SED differs (e.g., colder dust or different emissivity), the predicted fluxes and detection counts change.
domain assumption The CEERS HELM catalogue is representative of the HELM population over an arbitrary 1 deg^2 field at the same depth.
Invoked in Section 3 when scaling from 90 arcmin^2 to 1 deg^2. Cosmic variance and field-to-field differences are not quantified, and the extrapolation assumes the CEERS field is typical.
ad hoc to paper PRIMAger will reach the instrumental 5σ depths at λ > 42.6 µm despite confusion noise exceeding those depths.
Adopted in Section 3 for the S/N > 3 detection criterion. The paper's own text says confusion limits exceed the depths for λ > 42.6 µm, and the cited deblending work only demonstrates recovery to 281-7030 µJy at 96-235 µm, so this is an optimistic assumption unique to this paper.

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Cite this review

Pith. "Pith review of Sieging HELM's deep: PRIMA unveils the far-infrared properties of highly extincted low-mass galaxies." pith.science (2026). https://pith.science/paper/HIAWWEOU

@misc{pith2026250901305,
  author       = {Pith},
  title        = {Pith review of: Sieging HELM's deep: PRIMA unveils the far-infrared properties of highly extincted low-mass galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HIAWWEOU}},
  note         = {Machine review of arXiv:2509.01305}
}

abstract

Although the majority of star-forming galaxies show a tight correlation between stellar mass and dust extinction, recent James Webb Space Telescope observations have revealed a peculiar population of Highly Extincted Low-Mass (HELM) galaxies, which could revolutionise our understanding of dust production mechanisms. To fully understand the dust content of these galaxies, which are a minority of the overall galaxy population, far-infrared observations over large areas are pivotal. In this paper, we derive the expected PRIMAger, the far-IR (24-235$\mu m$) imaging camera proposed for the Probe far-IR Mission for Astrophysics, fluxes for a set of photometric candidates HELM galaxies. Taking into account a deep survey of 1000h over $1\rm\, deg^{2}$, we expect to detect around $3.1 \times 10^4$ HELM sources in at least one PRIMAger filter, 100 of which are at z=1-1.5. For 32% of this sample, there will be observations in at least four PRIMAger filters, covering at least the 90 to $240\mu m$ wavelength range, which will allow us to obtain a detailed fit of the dust emission and estimate the dust mass.

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Pith tools

Reviewed August 5, 2026 · model on record in the stance chip above.

[1] [1]

B. T. Draine , `` Interstellar Dust Grains ,'' 41 , 241--289 (2003)

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